[Skip to Content]

The SINGG and SUNGG surveys are star formation follow-up surveys of the HIPASS survey which imaged the whole southern sky in the light of 21cm radio emission line of neutral hydrogen, HI. While the optical and ultraviolet images of SINGG and SUNGG respectively allow galaxies to be studied at a resolution of 1 to 6 arcsec, the HIPASS HI data only has a resolution of 15 arcminutes (150 times poorer). Better resolution HI data exists for many of the galaxies in the SINGG and SUNGG surveys in the archives of the Very Large Array and the Australia Telescope Compact Array. This project will be to compile those data, obtained either in a reduced form from the original teams or in a raw form from the archives of the telescopes. The data will be processed to the stage of creating image cubes and mapping the distribution, velocity, and line width of HI.. Where practical rotation curves will be extracted, and mass models created. The data will be placed in a web accessible multi-wavelength database of SINGG and SUNGG observations. The end goal is to allow a multi-wavelength dissection of all luminous components of galaxies, and from mass models then determine the amount and distribution of the dark component. This subject is big enough to break into several different projects including:

  • Development of an ATCA HI data reduction pipeline: this would be well suited for a person that is adept with writing software and developing algorithms.
  • HI imaging of HI selected galaxy groups: this would be done in conjunction with V. Kilborn (Swinburne).
  • HI imaging of the MHONGOOSE precursor sample: This would be done in conjunction with E. de Blok (Astron, Cape Town)
NGC 2915 at optical (blue-green) & radio (red) wavelengths. Credit: HI data reduction: Ed Elson; Optical data acquisition and reduction: G. Meurer; HI data acquisition: W. J. G. de Blok.

Caption: The nearby blue compact dwarf galaxy NGC2915 as seen in HI (red) with the ATCA and the optical (cyan) with the CTIO 1.5m telescope. Credit: HI data reduction: Ed Elson; Optical data acquisition and reduction: G. Meurer; HI data acquisition: W. J. G. de Blok.